2007A&A...473..493B


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.06CET19:11:14

2007A&A...473..493B - Astronomy and Astrophysics, volume 473, 493-500 (2007/10-2)

The 105 L high-mass protostellar object IRAS23151+5912.

BEUTHER H., ZHANG Q., HUNTER T.R., SRIDHARAN T.K. and BERGIN E.A.

Abstract (from CDS):

While most sources above 105L have already formed an Ultracompact HII region (UCHII), this is not necessarily the case for sources of lower luminosity. Characterizing sources in the transition phase, i.e., very luminous objects without any detectable free-free emission, is important for a general understanding of massive star formation. We Characterize one of the most luminous High-Mass Protostellar Objects (HMPO) that has not yet formed any detectable UCHii region. The region was observed with the Submillimeter Array in three different array configurations at 875µm in the submm continuum and spectral line emission at sub-arcsecond resolution. The 875µm submm continuum emission has been resolved into at least two condensations. The previously believed driving source of one of the outflows, the infrared source IRS1, is ∼0.9'' offset from the main submm peak. The data do not allow to differentiate whether this offset is real, either caused by different sources or a shift of the photo-center due to scattering, or whether it is only due to poor astrometry of the infrared data. Over the entire 4GHz bandwidth we detect an intermediate dense spectral line forest with 27 lines from 8 different species, isotopologues or vibrationally-torsionally excited states. Temperature estimates based on the CH3OH line series result in values of T(Peak1)∼150±50K and T(Peak2)∼80±30K for the two submm peak positions, respectively. The SiO(8-7) red- and blue-shifted line maps indicate the presence of two molecular outflows. In contrast, the vibrationally-torsionally excited CH3OH line exhibits a velocity gradient approximately perpendicular to one of the outflows. With a size of approximately 5000AU and no Keplerian rotation signature, this structure does not resemble a genuine accretion disk but rather a larger-scale rotating toroid that may harbor a more common accretion disk at its so far unresolved center.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: early-type - stars: individual: IRAS23151+5912 - ISM: dust, extinction - ISM: jets and outflows

Nomenclature: Table 2, Fig.1: [BZH2007] Peak N (Nos 1-2).

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 7C 0059+5808 QSO 01 02 45.76238248 +58 24 11.1366009   20.09 19.22 18.57 17.90 ~ 197 1
2 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2051 1
3 IRAS 05358+3543 mul 05 39 10.4 +35 45 19           ~ 137 1
4 NAME SH 2-233 IR Cl* 05 39 10.4 +35 45 19           ~ 93 0
5 3C 279 Bla 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2752 2
6 GRS G012.89 +00.49 HII 18 11 51.3 -17 31 29           ~ 150 0
7 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 336 1
8 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 2037 1
9 3C 454.3 Bla 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2557 2
10 [BZH2007] Peak 2 smm 23 17 20.800 +59 28 47.17           ~ 1 0
11 [BZH2007] Peak 1 smm 23 17 20.916 +59 28 47.65           ~ 1 0
12 IRAS 23151+5912 HII 23 17 21.0 +59 28 49           ~ 93 0
13 [WBH2006] IRS 1 NIR ~ ~           ~ 4 0

    Equat.    Gal    SGal    Ecl

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